Spectral heterogeneity on Phobos and Deimos: HiRISE observations and comparisons to Mars Pathfinder results

Thomas, N.; Stelter, R. Deno; Ivanov, A. B.; Bridges, N. T.; Herkenhoff, K. E.; McEwen, A. S.

doi:10.1016/j.pss.2010.04.018

Cited by 51 publications

(37 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Processing of this image is described by Thomas et al . [] from three broadband filters with effective wavelengths being ~ R = 874 nm, G = 694 nm, and B = 536 nm.…”

Section: Space Weathering On the Moons Of Marsmentioning

confidence: 99%

Space weathering on airless bodies

2016

View full text Add to dashboard Cite

Space weathering refers to alteration that occurs in the space environment with time. Lunar samples, and to some extent meteorites, have provided a benchmark for understanding the processes and products of space weathering. Lunar soils are derived principally from local materials but have accumulated a range of optically active opaque particles (OAOpq) that include nanophase metallic iron on/in rims formed on individual grains (imparting a red slope to visible and near‐infrared reflectance) and larger iron particles (which darken across all wavelengths) such as are often found within the interior of recycled grains. Space weathering of other anhydrous silicate bodies, such as Mercury and some asteroids, produces different forms and relative abundance of OAOpq particles depending on the particular environment. If the development of OAOpq particles is minimized (such as at Vesta), contamination by exogenic material and regolith mixing become the dominant space weathering processes. Volatile‐rich bodies and those composed of abundant hydrous minerals (dwarf planet Ceres, many dark asteroids, and outer solar system satellites) are affected by space weathering processes differently than the silicate bodies of the inner solar system. However, the space weathering products of these bodies are currently poorly understood and the physics and chemistry of space weathering processes in different environments are areas of active research.

show abstract

“…Processing of this image is described by Thomas et al . [] from three broadband filters with effective wavelengths being ~ R = 874 nm, G = 694 nm, and B = 536 nm.…”

Section: Space Weathering On the Moons Of Marsmentioning

confidence: 99%

Space weathering on airless bodies

2016

View full text Add to dashboard Cite

show abstract

“…The CRISM Phobos data set consists of three observations acquired in succession on 23 October 2007 at an average phase angle of 41°, spatial sampling of 350 m/pixel, and covering approximately the same region in the western side of Phobos' sub‐Mars hemisphere (Table 1, Figure 2) [ Murchie et al , 2008]. HiRISE observations provide high‐resolution spatial context for the CRISM data, although the HiRISE data were not acquired in coordination with the CRISM data (Table 1, Figure 2) [ Thomas et al , 2011].…”

Section: Overview Of Data Setsmentioning

confidence: 99%

Analysis of disk‐resolved OMEGA and CRISM spectral observations of Phobos and Deimos

Fraeman¹,

Arvidson²,

Murchie³

et al. 2012

J. Geophys. Res.

View full text Add to dashboard Cite

[1] Disk-resolved observations of Phobos acquired by OMEGA at a range of lighting and viewing geometries were fit with the Hapke photometric function to solve for the single particle phase function and single scattering albedos from 0.4 to 2.5 mm. Single scattering albedos were recovered from CRISM observations of Phobos using the OMEGA derived single particle phase function and are similar to those from OMEGA data. Both the ubiquitous red unit and the blue unit around the crater Stickney exhibit a smooth red-sloped spectrum, with a steeper continuum in the redder unit. Single scattering albedos retrieved from CRISM measurements of Deimos are similar to those for the red unit on Phobos. Retrieval of single scattering albedos from OMEGA data at 2.8 to 5.0 mm has greater uncertainty, but results in this wavelength range are also consistent with a smooth, red-sloped spectrum. Phobos' and Deimos' low reflectances, lack of mafic absorption features, and red spectral slopes are incompatible with even highly space weathered chondritic or basaltic compositions. These results, coupled with similarities to laboratory spectra of Tagish Lake (possible D-type asteroid analog) and CM carbonaceous chondrite meteorites, show that Phobos and Deimos have primitive compositions. If the moons formed in situ rather than by capture of primitive bodies, primitive materials must have been added to the Martian system during accretion or a late stage impact.

show abstract

“…Multispectral observations reveal obvious effects of "space weathering" in areas where recent resurfacing is known to have exposed fresh material. Spacecraft spectral measurements for the surfaces of the satellites reveal two materials distinguished mainly by slope of the spectral continuum: a "redder" unit that dominates Deimos and is also present on Phobos, and a "bluer" unit excavated from depth on Phobos by the formation of Stickney crater (Murchie and Erard, 1996;Murchie et al, 1991;Rivkin et al, 2002;Thomas et al, 2011). Both Phobos' redder unit and Deimos indicate absorptions due to Fe-phyllosilicate near 0.65 µm (Murchie et al, 2008) and possibly olivine/pyroxene near 1 µm (Gendrin et al, 2005).…”

Section: Solar Wind Interactionmentioning

confidence: 99%

DePhine – The Deimos and Phobos Interior Explorer

Oberst

Wickhusen

Willner

et al. 2018

Advances in Space Research

View full text Add to dashboard Cite

DePhine -Deimos and Phobos Interior Explorer -is a mission proposed in the context of ESA's Cosmic Vision program, for launch in 2030. The mission will explore the origin and the evolution of the two Martian satellites, by focusing on their interior structures and diversity, by addressing the following open questions: Are Phobos and Deimos true siblings, originating from the same source and sharing the same formation scenario? Are the satellites rubble piles or solid bodies? Do they possess hidden deposits of water ice in their interiors? The DePhine spacecraft will be inserted into Mars transfer and will initially enter a Deimos quasi-satellite orbit to carry out a comprehensive global mapping. The goal is to obtain physical parameters and remote sensing data for Deimos comparable to data expected to be available for Phobos at the time of the DePhine mission for comparative studies. As a highlight of the mission, close flybys will be performed at low velocities, which will increase data integration times, enhance the signal strength and data resolution. 10 -20 flyby sequences, including polar passes, will result in a dense global grid of observation tracks. The spacecraft orbit will then be changed into a Phobos resonance orbit to carry out multiple close flybys and to perform similar remote sensing as for Deimos. The spacecraft will carry a suite of remote sensing instruments, including a camera system, a radio science experiment, a high-frequency radar, a magnetometer, and a Gamma Ray / Neutron Detector. A steerable antenna will allow simultaneous radio tracking and remote sensing observations (which is technically not possible for Mars Express). Additional instrumentation, e.g. a dust detector and a solar wind sensor, will address ---further science goals of the mission. If Ariane 6-2 and higher lift performance are available for launch (the baseline mission assumes a launch on a Soyuz Fregat), we expect to have greater spacecraft mobility and possibly added payloads.

show abstract

Spectral heterogeneity on Phobos and Deimos: HiRISE observations and comparisons to Mars Pathfinder results

Cited by 51 publications

References 29 publications

Space weathering on airless bodies

Space weathering on airless bodies

Analysis of disk‐resolved OMEGA and CRISM spectral observations of Phobos and Deimos

DePhine – The Deimos and Phobos Interior Explorer

Contact Info

Product

Resources

About